SIMBAD references

2020A&A...644A.112H - Astronomy and Astrophysics, volume 644A, 112-112 (2020/12-1)

An extreme particle accelerator in the Galactic plane: HESS J1826-130.

HESS COLLABORATION, ABDALLA H., ADAM R., AHARONIAN F., AIT BENKHALI F., ANGUNER E.O., ARCARO C., ARMAND C., ARMSTRONG T., ASHKAR H., BACKES M., BAGHMANYAN V., BARBOSA MARTINS V., BARNACKA A., BARNARD M., BECHERINI Y., BERGE D., BERNLOHR K., BI B., BOTTCHER M., BOISSON C., BOLMONT J., DE BONY DE LAVERGNE M., BORDAS P., BREUHAUS M., BRUN F., BRUN P., BRYAN M., BUCHELE M., BULIK T., BYLUND T., CAROFF S., CAROSI A., CASANOVA S., CHAND T., CHANDRA S., CHEN A., COTTER G., CURYLO M., DAMASCENE MBARUBUCYEYE J., DAVIDS I.D., DAVIES J., DEIL C., DEVIN J., DEWILT P., DIRSON L., DJANNATI-ATAI A., DMYTRIIEV A., DONATH A., DOROSHENKO V., DUFFY C., DYKS J., EGBERTS K., EICHHORN F., EINECKE S., EMERY G., ERNENWEIN J.-P., FEIJEN K., FEGAN S., FIASSON A., FICHET DE CLAIRFONTAINE G., FONTAINE G., FUNK S., FUSSLING M., GABICI S., GALLANT Y.A., GIAVITTO G., GIUNTI L., GLAWION D., GLICENSTEIN J.F., GOTTSCHALL D., GRONDIN M.-H., HAHN J., HAUPT M., HERMANN G., HINTON J.A., HOFMANN W., HOISCHEN C., HOLCH T.L., HOLLER M., HORBE M., HORNS D., HUBER D., JAMROZY M., JANKOWSKY D., JANKOWSKY F., JARDIN-BLICQ A., JOSHI V., JUNG-RICHARDT I., KASAI E., KASTENDIECK M.A., KATARZYNSKI K., KATZ U., KHANGULYAN D., KHELIFI B., KLEPSER S., KLUZNIAK W., KOMIN N., KONNO R., KOSACK K., KOSTUNIN D., KRETER M., LAMANNA G., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LEVY C., LOHSE T., LYPOVA I., MACKEY J., MAJUMDAR J., MALYSHEV D., MALYSHEV D., MARANDON V., MARCHEGIANI P., MARCOWITH A., MARES A., MARTI-DEVESA G., MARX R., MAURIN G., MEINTJES P.J., MEYER M., MITCHELL A., MODERSKI R., MOHAMED M., MOHRMANN L., MONTANARI A., MOORE C., MORRIS P., MOULIN E., MULLER J., MURACH T., NAKASHIMA K., NAYERHODA A., DE NAUROIS M., NDIYAVALA H., NIEDERWANGER F., NIEMIEC J., OAKES L., O'BRIEN P., ODAKA H., OHM S., OLIVERA-NIETO L., DE ONA WILHELMI E., OSTROWSKI M., OYA I., PANTER M., PANNY S., PARSONS R.D., PERON G., PEYAUD B., PIEL Q., PITA S., POIREAU V., PRIYANA NOEL A., PROKHOROV D.A., PROKOPH H., PUHLHOFER G., PUNCH M., QUIRRENBACH A., RAAB S., RAUTH R., REICHHERZER P., REIMER A., REIMER O., REMY Q., RENAUD M., RIEGER F., RINCHIUSO L., ROMOLI C., ROWELL G., RUDAK B., RUIZ-VELASCO E., SAHAKIAN V., SAILER S., SANCHEZ D.A., SANTANGELO A., SASAKI M., SCALICI M., SCHUSSLER F., SCHUTTE H.M., SCHWANKE U., SCHWEMMER S., SEGLAR-ARROYO M., SENNIAPPAN M., SEYFFERT A.S., SHAFI N., SHININGAYAMWE K., SIMONI R., SINHA A., SOL H., SPECOVIUS A., SPENCER S., SPIR-JACOB M., STAWARZ L., SUN L., STEENKAMP R., STEGMANN C., STEINMASSL S., STEPPA C., TAKAHASHI T., TAVERNIER T., TAYLOR A.M., TERRIER R., TIZIANI D., TLUCZYKONT M., TOMANKOVA L., TRICHARD C., TSIROU M., TUFFS R., UCHIYAMA Y., VAN DER WALT D.J., VAN ELDIK C., VAN RENSBURG C., VAN SOELEN B., VASILEIADIS G., VEH J., VENTER C., VINCENT P., VINK J., VOLK H.J., VUILLAUME T., WADIASINGH Z., WAGNER S.J., WATSON J., WERNER F., WHITE R., WIERZCHOLSKA A., WONG Y.W., YUSAFZAI A., ZACHARIAS M., ZANIN R., ZARGARYAN D., ZDZIARSKI A.A., ZECH A., ZHU S.J., ZIEGLER A., ZORN J., ZOUARI S. and ZYWUCKA N.

Abstract (from CDS):

The unidentified very-high-energy (VHE; E>0.1TeV) γ-ray source, HESS J1826-130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215h of HESS data has revealed a steady γ-ray flux from HESS J1826-130, which appears extended with a half-width of 0.21°±0.02_stat°± 0.05_sys°. The source spectrum is best fit with either a power-law function with a spectral index Γ=1.78±0.10_stat± 0.20_sys and an exponential cut-off at 15.2_–3.2^+5.5TeV, or a broken power-law with Γ₁=1.96±0.06_stat±0.20_sys, Γ₂=3.59±0.69_stat±0.20_sys for energies below and above E_br=11.2±2.7TeV, respectively. The VHE flux from HESS J1826-130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula, HESS J1825-137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826-130 VHE emission related to PSR J1826-1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826-130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to ≥200TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants, molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.

Abstract Copyright: © H.E.S.S. Collaboration 2020

Journal keyword(s): ISM: supernova remnants - ISM: clouds - gamma rays: general - gamma rays: ISM

Simbad objects: 12

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